Spectropolarimetric evidence for a siphon flow along an emerging magnetic flux tube
| Autor: | B. Ruiz Cobo, Sami K. Solanki, J. Blanco Rodríguez, M. van Noort, J. C. del Toro Iniesta, W. Schmidt, D. Orozco Suárez, Laurent Gizon, M. Knölker, Iker S. Requerey, V. Martínez Pillet, Peter Barthol, Johann Hirzberger, Achim Gandorfer, Tino L. Riethmüller |
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| Přispěvatelé: | Ministerio de Economía y Competitividad (España), Max Planck Society, National Science Foundation (US), National Aeronautics and Space Administration (US), National Research Foundation of Korea |
| Jazyk: | angličtina |
| Rok vydání: | 2017 |
| Předmět: |
010504 meteorology & atmospheric sciences
Polarity (physics) photosphere [Sun] FOS: Physical sciences Astrophysics polarimetric [Techniques] 01 natural sciences Methods: observational 0103 physical sciences Sunrise Astrophysics::Solar and Stellar Astrophysics observational [Methods] 010303 astronomy & astrophysics Sun: magnetic fields Solar and Stellar Astrophysics (astro-ph.SR) 0105 earth and related environmental sciences Line (formation) Physics Solar observatory Polarity symbols Techniques: polarimetric Sun: photosphere Astronomy and Astrophysics Magnetic flux Magnetic field Astrophysics - Solar and Stellar Astrophysics Flow (mathematics) magnetic fields [Sun] Space and Planetary Science |
| Zdroj: | Digital.CSIC. Repositorio Institucional del CSIC instname |
| Popis: | ©2017 The American Astronomical Society. All rights reserved.We study the dynamics and topology of an emerging magnetic flux concentration using high spatial resolution spectropolarimetric data acquired with the Imaging Magnetograph eXperiment on board the sunrise balloon-borne solar observatory. We obtain the full vector magnetic field and the line of sight (LOS) velocity through inversions of the Fe i line at 525.02 nm with the SPINOR code. The derived vector magnetic field is used to trace magnetic field lines. Two magnetic flux concentrations with different polarities and LOS velocities are found to be connected by a group of arch-shaped magnetic field lines. The positive polarity footpoint is weaker (1100 G) and displays an upflow, while the negative polarity footpoint is stronger (2200 G) and shows a downflow. This configuration is naturally interpreted as a siphon flow along an arched magnetic flux tube. This work has been partially funded by the Spanish Ministerio de Economía y Competitividad, through Projects No. ESP2013-47349-C6 and ESP2014-56169-C6, including a percentage from European FEDER funds. The German contribution to sunrise and its reflight was funded by the Max Planck Foundation, the Strategic Innovations Fund of the President of the Max Planck Society (MPG), DLR, and private donations by supporting members of the Max Planck Society, which is gratefully acknowledged. The National Solar Observatory (NSO) is operated by the Association of Universities for Research in Astronomy (AURA) Inc. under a cooperative agreement with the National Science Foundation. The HAO contribution was partly funded through NASA grant number NNX13AE95G. This work was partly supported by the BK21 plus program through the National Research Foundation (NRF) funded by the Ministry of Education of Korea. |
| Databáze: | OpenAIRE |
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